Evolution of protoplanetary disks: constraints from DM Tauri and GM Aurigae

R. Hueso; T. Guillot

doi:doi:10.1051/0004-6361:20041905

Free access

Issue		A&A Volume 442, Number 2, November I 2005


Page(s)		703 - 725
Section		Planets and planetary systems
DOI		http://dx.doi.org/10.1051/0004-6361:20041905

A&A 442, 703-725 (2005)
DOI: 10.1051/0004-6361:20041905

Evolution of protoplanetary disks: constraints from DM Tauri and GM Aurigae

R. Hueso¹ and T. Guillot²

¹ Física Aplicada I, ETS Ing. Universidad del País Vasco, Alda. Urquijo s/n, 48013 Bilbao, Spain
e-mail: wubhualr@lg.ehu.es
² Laboratoire Cassiopée, CNRS UMR 6202, Observatoire de la Côte d'Azur, Nice, France
e-mail: guillot@obs-nice.fr

(Received 26 August 2004 / Accepted 21 June 2005 )

Abstract
We present a one-dimensional model of the formation and viscous evolution of protoplanetary disks. The formation of the early disk is modeled as the result of the gravitational collapse of an isothermal molecular cloud. The disk's viscous evolution is integrated according to two parameterizations of turbulence: the classical $\alpha$ representation and a $\beta$ parameterization, representative of non-linear turbulence driven by the keplerian shear. We apply the model to DM Tau and GM Aur, two classical T-Tauri stars with relatively well-characterized disks, retrieving the evolution of their surface density with time. We perform a systematic Monte-Carlo exploration of the parameter space (i.e. values of the $\alpha$ - $\beta$ parameters, and of the temperature and rotation rate in the molecular cloud) to find the values that are compatible with the observed disk surface density distribution, star and disk mass, age and present accretion rate. We find that the observations for DM Tau require $0.001<\alpha<0.1$ or $2\times 10^{-5}<\beta<5\times 10^{-4}$ . For GM Aur, we find that the turbulent viscosity is such that $4\times 10^{-4}<\alpha<0.01$ or $2\times 10^{-6}<\beta<8\times 10^{-5}$ . These relatively large values show that an efficient turbulent diffusion mechanism is present at distances larger than ~ $10\,$ AU. This is to be compared to studies of the variations of accretion rates of T-Tauri stars versus age that mostly probe the inner disks, but also yield values of $\alpha\sim 0.01$ . We show that the mechanism responsible for turbulent diffusion at large orbital distances most probably cannot be convection because of its suppression at low optical depths.

Key words: accretion, accretion disks -- solar system: formation -- planetary systems: formation -- planetary systems: protoplanetary disks

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